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J/ApJ/700/1173     Analysis of broad-line regions in AGNs           (Zhu+, 2009)

Evidence for an intermediate line region in active galactic nuclei's inner torus region and its evolution from narrow to broad line Seyfert I galaxies. Zhu L., Zhang S.N., Tang S. <Astrophys. J., 700, 1173-1189 (2009)> =2009ApJ...700.1173Z
ADC_Keywords: Active gal. nuclei ; Models ; Line Profiles Keywords: galaxies: active - galaxies: nuclei - galaxies: structure - Galaxy: evolution - line: profiles - quasars: emission lines Abstract: A two-component model for the broad-line region (BLR) of active galactic nuclei (AGNs) has been suggested for many years but not widely accepted. This model indicates that the broad line can be described with the superposition of two Gaussian components (very broad Gaussian component (VBGC) and intermediate Gaussian component (IMGC)) which are from two physically distinct regions, i.e., very broad line region (VBLR) and intermediate line region. We select a Sloan Digital Sky Survey sample to further confirm this model and give a detailed analysis of the geometry, density, and evolution of these two regions. Description: The sample contains 90 objects with clear Hα, Hβ, and Hγ line profiles that can be decomposed. They are selected by La Mura et al. (2007ApJ...671..104L) from SDSS 3 based on their Balmer line intensities. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 123 90 Source properties and decomposition parameters
See also: J/ApJ/613/682 : AGN central masses and broad-line region sizes (Peterson+, 2004) J/ApJ/660/1072 : Unified model of active galactic nuclei (Wang+, 2007) J/MNRAS/383/581 : Broad-line Balmer decrements in blue AGN (Dong+, 2008) J/ApJ/690/20 : Models of the AGN and black hole populations (Shankar+, 2009) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Seq Running sequence number 4- 7 A4 --- --- [SDSS] 8- 17 A10 --- Name Object name (JHHMM+DDMM) 19- 23 F5.3 --- z Redshift from La Mura G., private com. (1) 25- 30 F6.2 10+35W L5100 ? Continuum luminosity at the rest frame wavelength of 5100Å in units of 1042erg/s (2) 32- 38 F7.2 10+5Msun BHMass ? Black hole mass in 10^5^M_sun_ units (2) 40- 45 F6.2 --- Ha.b ? Hα lines: Hb (height of the VBGC (very broad Gaussian component)) 47- 51 F5.1 --- Ha.i ? Hα lines: Hi (height of the IMGC (intermediate Gaussian component)) 53- 56 I4 km/s W(Ha) ? Hα lines: FWHM 58- 61 I4 km/s Wb(Ha) ? Hα lines: FWHM of broad component 63- 66 I4 km/s Wi(Ha) ? Hα lines: FWHM of intermediate comp. 68- 73 F6.2 --- Hb.b ? Hβ lines: Hb (height of the VBGC) 75- 80 F6.2 --- Hb.i ? Hβ lines: Hi (height of the IMGC) 82- 85 I4 km/s W(Hb) ? Hβ lines: FWHM 87- 90 I4 km/s Wb(Hb) ? Hβ lines: FWHM of broad component 92- 95 I4 km/s Wi(Hb) ? Hβ lines: FWHM of intermediate comp. 97-102 F6.2 --- Hg.b ? Hγ lines: Hb (height of the VBGC) 104-108 F5.2 --- Hg.i ? Hγ lines: Hi (height of the IMGC) 110-113 I4 km/s W(Hg) ? Hγ lines: FWHM 115-118 I4 km/s Wb(Hg) ? Hγ lines: FWHM of broad component 120-123 I4 km/s Wi(Hg) ? Hγ lines: FWHM of intermediate comp.
Note (1): Reshifts in this column are not associated with the good SDSS identifications. This mix-up parameter does not affect the other data. Note (2): From La Mura et al. 2007ApJ...671..104L
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 26-Jul-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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